Pith. sign in

REVIEW 4 major objections 5 minor 2 cited by

Little Red Dots from Small-Scale Primordial Black Hole Clustering

T0 review · 4 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Clustered populations of light primordial black holes can grow into the million-solar-mass seeds inferred in little red dots by redshift six.

desk verdict A promising proof-of-concept for LRD seeds from clustered PBH mergers, but the printed clustering formula in the supplement undercuts the paper's own fiducial parameters—fixable, but load-bearing. read the letter →

arxiv 2507.07171 v2 pith:TRSYC3HT submitted 2025-07-09 astro-ph.CO astro-ph.GAgr-qchep-ph

Borui Zhang , Wei-Xiang Feng , Haipeng An This is my paper
classification astro-ph.COastro-ph.GAgr-qchep-ph
keywords littlereddotsprimordialblackholesPBHclusteringlong-shortmodecouplingsupermassiveholeseedsrunawaymergersstochasticgravitationalwavebackgroundCMBspectraldistortions
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper proposes that the supermassive black holes powering JWST's little red dots can grow from dense clusters of light primordial black holes, rather than from the direct collapse of rare, heavy perturbations. It argues that long-wavelength modulations of the short-wavelength density field, with coupling $|\eta| \sim 14$, produce clusters of about $10^5$ black holes of $30\,M_\odot$ with number density $\sim 2\times10^8\,\mathrm{pc}^{-3}$, and that within these clusters two-body mergers run away to build a $\sim 10^6\,M_\odot$ black hole by $z \simeq 6$. This route sidesteps the cosmic microwave background spectral distortion bounds that exclude heavy direct-collapse seeds, produces black holes born with near-maximal spin from the cluster's tidal spin residual, and predicts a stochastic gravitational-wave background with two peaks. If the mechanism operates, it explains both the heavy seeds and the high spins inferred for little red dots.

What carries the argument

The load-bearing mechanism is the long-short mode coupling of Eq. (4), $\nu(x) = \nu_g(1 + \eta\Phi_l(x))$, which spatially modulates the PBH formation threshold and produces clusters whose two-point correlation is $\xi_\alpha \simeq \delta_c\eta\kappa$ out to the long-mode scale $r_{\rm cl} \sim 1/k_l$. This clustering fixes the initial conditions: number density $n_{\rm cl} \simeq 2\times10^8\,\mathrm{pc}^{-3}$ for $f_{\rm pbh}\xi_\alpha/25 \simeq 1$, compactness $C=20$, and $m_{\rm pbh}=30\,M_\odot$, with cluster mass $M_{\rm cl}\propto r_{\rm cl}^3$. Inside the cluster, the Smoluchowski coagulation equation (Eq. 10) with the velocity-averaged gravitational-radiation merger kernel $K_{ij}$ (Eq. 11) tracks the mass population; the controlling rate is the runaway timescale $t_{\rm rm} \simeq 0.2/(n_{\rm cl}K_{00})$, which must be below about a gigayear for the seed to appear by $z\gtrsim5$. The spin is supplied by the quadrupole tidal-torque model: an ellipsoidal cluster in the tidal field of neighbours accumulates angular momentum before merging, giving a residual spin that reaches the Kerr limit.

What would settle it

A decisive check is a cosmological simulation of PBH formation under Eq. (4) with $\nu_g=8.5$, $\kappa=0.1313$, and $|\eta|\simeq14$; it would show whether clusters with $\xi_\alpha\sim10^6$, compactness $C=20$, and virial radius $r_{\rm vir}\simeq0.05$ pc actually form rather than collapsing directly or dispersing. On the observational side, a null detection of the predicted two-peaked stochastic gravitational wave background at the amplitudes of Fig. 3 by next-generation interferometers would exclude $n_{\rm cl}=2\times10^8\,\mathrm{pc}^{-3}$ clusters for $N_{\rm cl}=10^5$, $30\,M_\odot$ PBHs.

Watch

Extended reading notes

Core claim

The central claim is that a supermassive black hole of $\sim 10^6\,M_\odot$ emerges by redshift $z \sim 6$ from the runaway merger of $N_{\rm cl} = 10^5$ monochromatic primordial black holes of $m_{\rm pbh} = 30\,M_\odot$ in a cluster with number density $n_{\rm cl} = 2\times10^8\,\mathrm{pc}^{-3}$ and virial velocity $v_{\rm vir} = 512\,\mathrm{km}\,\mathrm{s}^{-1}$. The cluster originates from long-short mode coupling described by $\nu(x) = \nu_g (1 + \eta \Phi_l(x))$ with $\nu_g = 8.5$, $|\eta| \simeq 14$, and $\kappa \equiv \sigma_l/\bar\sigma_s \simeq 0.13$; this yields a nearly flat PBH two-point correlation $\xi_\alpha \sim 10^6$ on cluster scales and a PBH fraction $f_{\rm pbh} \sim 10^{-5}$. The merger cascade, solved by Monte Carlo simulation of the Smoluchowski coagulation equation, proceeds in three stages: small-mass mergers at high redshift, intermediate-mass mergers that accelerate the process, and finally inspirals of the remaining PBHs onto the growing central hole. The resulting black hole inherits a near-maximal spin from the cluster's tidal-field angular momentum, and the whole process generates a two-peaked stochastic gravitational wave background.

Load-bearing premise

The load-bearing premise is that the early universe's long- and short-wavelength density fluctuations are coupled strongly enough (roughly $|\eta|\sim14$ with threshold $\nu_g=8.5$) to pack primordial black holes into clusters with a million-fold density enhancement, an abundance of about $10^{-5}$ of dark matter, and a post-collapse compactness factor of $C=20$, so that the cluster density reaches $\sim2\times10^8\,\mathrm{pc}^{-3}$; if no real mechanism delivers that packing, the runaway-merger channel and its black-hole and gravitational-wave predictions fail.

Editorial extensions

If this is right

  • If the mechanism is right, little red dots do not require heavy direct-collapse seeds: clustered $30\,M_\odot$ PBHs produce $10^{5-8}\,M_\odot$ black holes by $z\simeq4$–$11$, with or without later gas accretion.
  • The CMB $\mu$- and $y$-distortion bounds are evaded because the long-mode variance is kept small, $\sigma_l\lesssim0.0064$, while $f_{\rm pbh}\sim10^{-5}$ still matches the locally inferred SMBH mass density.
  • Because the merged seed is born nearly maximally spinning, its radiative efficiency is high ($\epsilon_M\simeq0.42$ for $a_\bullet\simeq1$), which suppresses later Eddington growth and is consistent with a slow-growth, obscured-AGN reading of LRD luminosity.
  • The stochastic gravitational wave background from the three merger stages has two spectral peaks and an infrared tail scaling as $f^3$, steeper than the $f^{2/3}$ of single inspirals, giving next-generation detectors a discriminating signature.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Editorial inference: a population-level spin test follows: the cluster-merger channel predicts many LRD black holes born with $a_\bullet\simeq1$, whereas steady gas-disk growth saturates near $a_\bullet\simeq0.95$ (MHD) or lower after chaotic accretion, so a high-spin excess at $z>4$ would favour this origin.
  • Editorial inference: the two-peak gravitational wave template could be searched for in combined space-borne and terrestrial data; a detection would independently measure $\xi_\alpha\sim10^6$ clustering even if individual extreme-mass-ratio inspirals are not resolved.
  • Editorial inference: the paper fixes $\nu_g=8.5$ and $|\eta|\sim14$ by hand; the open test is whether any complete inflation or phase-transition model generates this combination without violating CMB constraints, which a dedicated model-building study could provide.
  • Editorial inference: replacing the homogeneous-ellipsoid tidal model with cosmological $N$-body simulations of clustered PBH formation would quantify the spin distribution and the fraction of clusters that avoid immediate collapse, sharpening the predicted LRD black hole spin distribution.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

4 major / 5 minor

Summary. The paper proposes that clusters of ~30 M☉ primordial black holes (PBHs), created by long-short wavelength mode coupling on small scales, can undergo runaway mergers described by the Smoluchowski coagulation equation and produce ~10^6 M☉ supermassive black holes by z~6, thereby offering a heavy-seed explanation for the little red dots observed by JWST. The cluster properties are derived from the PBH two-point correlation function, the merger evolution is simulated with a Monte Carlo scheme, and the model is shown to evade CMB µ-distortion bounds while predicting a two-peak stochastic gravitational wave background. The paper also argues that tidal interactions give the resulting black holes a high spin.

Significance. If the mechanism works, it is a plausible and falsifiable route to heavy, rapidly spinning black hole seeds at high redshift without violating CMB spectral distortion constraints, and it produces a distinctive GW signature. The analytic scaling in Eq. (3) is useful, and the Monte Carlo coagulation approach is physically motivated. The paper is explicit that it is a proof of concept and that some ingredients, notably the infrared f^3 GW scaling and the effect of mass segregation, are deferred to a companion paper (Ref. [71]), which limits independent verification. The central difficulty is that the printed clustering formula in the Supplemental Material does not reproduce the ξα ~ 10^6 value used throughout, and the simulation is a single run without error bars, so the headline claims rest on an internally inconsistent input.

major comments (4)
  1. [Appendix S.1, Eq. (S.1-4)] The printed two-point correlation formula does not reproduce the value ξα ~ 10^6 quoted in the text for the fiducial parameters. With ν_g = 8.5, κ = 0.1313, and |η| = 14.34, we obtain α = δc η κ ≈ 0.779, ω̄ = α^2/(1+α^2) ≈ 0.378, so the exponent in Eq. (S.1-4) is ν_g^2 ω̄/(1+ω̄) ≈ 19.8, yielding 1+ξ ≈ 8×10^8, i.e., ξα ~ 10^9. This contradicts the value ξα ~ 10^6 used in Eqs. (8)-(9) and in Fig. 3. The resolution appears to be that the threshold of the combined field should be reduced by √(1+α^2), replacing ν_g^2 in the exponent by ν_g^2/(1+α^2), which gives exponent ≈ 12.3 and ξα ~ several ×10^5, consistent with the fiducial parameters. As written, Eq. (S.1-4) is missing this suppression, and since Eq. (8) depends on (f_pbh ξα)^4, the error is load-bearing. The authors must correct the formula or justify a different definition of α.
  2. [Runaway Mergers, Eq. (3) vs. Fig. 2] The analytic estimate in Eq. (3) states that n_cl ≳ 3×10^9 pc^-3 is required for the emergence of a ~10^6 M☉ SMBH within the first billion years. However, the Monte Carlo simulation in Fig. 2 uses n_cl = 2×10^8 pc^-3 (with N_cl = 10^5, m_pbh = 30 M☉, M_cl = 3×10^6 M☉, r_vir ≈ 0.05 pc) and produces M• ~ 10^6 M☉ by z ~ 6. For these parameters Eq. (3) gives t_merg ≈ 8 Gyr, more than an order of magnitude longer than the simulation's ~0.6 Gyr. The text says Eq. (3) is 'conservative', but the discrepancy is large enough that the claimed threshold is misleading. The authors should explicitly relate t_merg (the half-coalescence timescale) to the runaway timescale t_rm and explain why the simulation is consistent with the analytic estimate.
  3. [Fig. 3 and GW background] The predicted stochastic GW background for the fiducial parameters (f_pbh = 5.66×10^-5, n_cl = 2×10^8 pc^-3, v_vir = 512 km/s) appears to reach Ω_gw h^2 values that exceed the current aLIGO+VIRGO upper limits in the LIGO band, yet the paper does not compare against these non-detection bounds. If the curves are correctly normalized, this would rule out the model rather than provide a signature. The authors should state the current upper limits explicitly and show that the predicted spectrum is consistent with them, or explain why the normalization is not directly comparable. In addition, the claimed infrared f^3 scaling is attributed to Ref. [71] (in preparation); without a derivation or an accessible reference, this key signature cannot be independently assessed.
  4. [Monte Carlo simulation (Fig. 2 and Fig. 3)] The central quantitative results—the emergence of a ~10^6 M☉ SMBH by z~6 and the GW spectra—are presented as a single Monte Carlo realization with no error bars, no convergence tests with respect to the number of particles or timestep, and no statement of the number of realizations. Given that the fiducial parameters are hand-picked to produce the desired outcome, the robustness of the runaway-merger timescale is not yet established. The authors should provide at least a convergence check or a statistical uncertainty estimate, or explicitly state that the figure shows one representative realization.
minor comments (5)
  1. [Eq. (7)] The expression for β(m_pbh) is written as erfc(ν_g/√2 1/√(1+α^2)), which is ambiguous; it should be written as erfc[ν_g/√(2(1+α^2))] or with explicit parentheses.
  2. [Fig. 2] The label 'm_i=33 /m_pbh = 33' in the second panel appears to be a typo; it should presumably read 'm_i/m_pbh = 33' or similar.
  3. [Spin argument, Eq. (13) and text after it] The claim that the cluster spin parameter a_cl exceeding the Kerr limit implies a nearly maximal black hole spin a• ~ 1 is not derived. The mapping from the cluster angular momentum to the spin of the final merger product, including any angular momentum losses during runaway mergers, should be discussed.
  4. [Fig. 1 and Discussion] The legend of Fig. 1 labels several regions (light-gray, green, purple, darker band) but the figure itself does not identify them; the reader has to match them from the text. Adding a legend or labels would improve clarity.
  5. [Throughout] The notation for the PBH fraction f_pbh and the correlation ξα is used interchangeably with the combination f_pbh ξα; please define the combination once and use it consistently.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the runaway-merger SMBH is a forward Monte Carlo result from cluster parameters, not a fitted recasting of the target.

full rationale

The paper's central chain is: choose a long-short mode coupling (nu_g = 8.5, |eta| ~ 14), compute the resulting PBH abundance f_pbh and clustering amplitude xi_alpha from Eqs. 6-7 and S.1-4, set cluster properties (n_cl, M_cl, r_vir, v_vir) from Eqs. 8-9, then evolve the mass distribution with the Smoluchowski coagulation equation (Eq. 10) using an external Monte Carlo method. The final M_bullet ~ 10^6 M_sun by z ~ 6 is an output of that evolution for the chosen input cluster, not a parameter fitted to LRD masses; the text carefully says the mechanism 'can explain' LRDs, and Fig. 2 shows the population evolution rather than imposing the final mass. The parameters f_pbh ~ 10^-5 and xi_alpha ~ 10^6 are inputs selected for viability, not predictions masquerading as derivations. The only self-citations are Ref. [27] (published, with a co-author) for the binary periapsis formula and Ref. [71] ('In preparation') for the infrared f^3 scaling of the GW spectrum and the possible mass-segregation speed-up; these support secondary signatures and conservativeness statements, while the SMBH-formation claim is computed in the paper itself. The skeptic's concern that the printed Eq. S.1-4 yields xi_alpha ~ 10^9 rather than 10^6 would be an internal numerical or typographical inconsistency, not a circularity: it does not make the downstream computation equivalent to its inputs by construction. No load-bearing circular step is identifiable.

Assumptions & free parameters 8 free parameters · 6 assumptions · 0 invented entities

The model is a proof of concept whose central outputs, namely cluster density, SMBH mass, spin, and GW spectrum, are controlled by the hand-chosen parameters nu_g, eta, kappa, k_l/k_s, C and m_pbh. The merger dynamics themselves are simulated, but the initial conditions are tuned to make the scenario work. No new particles, forces, or exotic fields are introduced, so the invented-entity ledger is empty.

free parameters (8)
  • nu_g (reduced short-mode threshold) = 8.5
    Set by hand in the paragraph 'In this study, we fix nu_g = 8.5...' to make clustering large enough and PBH abundance around 10^-5. It sets sigma_s ~ 0.0487 and, through Eqs.6-8, the cluster density.
  • |eta| (long-short mode coupling strength) = ~14 (14.34 in fiducial)
    Chosen to reach xi_alpha ~ 10^6 and f_pbh ~ 5.66 x 10^-5. The light-gray LRD-allowed region in Fig.1 depends on this value.
  • kappa = sigma_l / sigma_s = 0.1313 (sigma_l ~ 0.0064)
    Chosen so the long-mode variance evades CMB mu-distortion constraints while still contributing to the clustering signal.
  • k_l / k_s (wavenumber ratio) = ~10^-4
    Sets r_cl ~ 10 kpc, M_cl ~ 3 x 10^6 solar masses, r_vir ~ 0.05 pc and v_vir ~ 500 km/s in the fiducial case; controls the final SMBH mass scale through Eq.9.
  • C (compactness parameter) = 20
    Adopted in Eq.8 to set n_cl ~ 2 x 10^8 pc^-3 after virialization. A different C changes the merger rate and all timescales.
  • f_pbh (PBH fraction of dark matter) = 5.66 x 10^-5
    Target abundance for the fiducial spectrum; emerges from nu_g and eta via Eqs.6-7 and is matched to the local SMBH mass density rho_bullet ~ 10^5 solar masses Mpc^-3.
  • H(e,p) cluster shape factor = 0.53
    Average non-sphericity from peak theory with e_bar = 0.09 and p_bar = 0; enters Eq.13 and determines whether the predicted spin parameter exceeds the Kerr limit.
  • m_pbh (initial PBH mass) = 30 solar masses
    Model choice tied to k_s ~ 2.5 pc^-1. O(10) solar mass PBHs are weakly constrained, and the final SMBH mass scales with this input.
assumptions (6)
  • domain assumption Both long and short mode density fields are Gaussian, and PBH formation is modulated as nu(x) = nu_g (1 + eta Phi_l(x))
    Eq.4 and Supplement S.1. This is the origin of xi_alpha ~ 10^6, and the required eta ~ 14 and nu_g = 8.5 are not derived from a specific inflationary model.
  • domain assumption PBH abundance beta and f_pbh follow Eqs.6-7 from Refs. [20,21,24]
    These formulas convert the modulated threshold into f_pbh ~ 10^-5; the entire cluster population estimate depends on them.
  • domain assumption The cluster decouples before matter-radiation equality, virializes with compactness C = 20, and freezes its comoving number density n_cl = C (0.85 f_pbh xi_alpha)^4 rho_eq / m_pbh
    Supplement S.2, Eqs.S.2-5 and S.2-6. This produces the extreme n_cl ~ 2 x 10^8 pc^-3 that drives the runaway merger.
  • domain assumption Two-body gravitational-wave capture dominates mergers, with kernel K_ij from Mouri-Taniguchi, while three-body disruption and mass segregation are neglected
    Eqs.10-11 and Supplement S.5. The simulation and the runaway timescale are direct outputs of this assumption.
  • domain assumption PBH clusters are homogeneous ellipsoids and acquire spin from quadrupole tidal torques exerted by neighboring clusters, with average ellipticity e_bar = 0.09
    Supplement S.3, Eqs.S.3-7 to S.3-10. The high-spin prediction is based on this analytic model, not on a full merger simulation.
  • ad hoc to paper The stochastic GW background and its f^3 infrared scaling are as described in Ref. 71, an in-preparation paper by the same authors
    Fig.3 and the accompanying text; the derivation is not present in this preprint, so the GW prediction rests on an unpublished self-citation.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Little Red Dots from Small-Scale Primordial Black Hole Clustering." pith.science (2026). https://pith.science/paper/TRSYC3HT

@misc{pith2026250707171,
  author       = {Pith},
  title        = {Pith review of: Little Red Dots from Small-Scale Primordial Black Hole Clustering},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/TRSYC3HT}},
  note         = {Machine review of arXiv:2507.07171}
}
abstract

The James Webb Space Telescope (JWST) observations have identified a class of compact galaxies at high redshifts ($4 \lesssim z \lesssim 11$), dubbed "little red dots" (LRDs). The supermassive black holes (SMBHs) of $10^{5-8}{\rm\,M}_{\odot}$ in LRDs favor a heavy-seed origin. We propose a mechanism for their formation: Clusters of primordial black holes, formed through long-short mode coupling on small scales in the early Universe, undergo sequential mergers over extended timescales. This mechanism can evade cosmic microwave background distortions and result in heavy-seed SMBHs via runaway mergers. We employ Monte Carlo simulations to solve the Smoluchowski coagulation equation and determine the runaway merging timescale. The resulting stochastic gravitational wave background offers a distinct signature of this process, and the forming SMBHs can be highly spinning at their formation due to the spin residual of the cluster from tidal fields. This mechanism may explain the rapidly spinning SMBHs in LRDs under the assumption of obscured active galactic nuclei.

Figures

Figures reproduced from arXiv: 2507.07171 by the authors.

Figure 1
Figure 1. summarizes the parameter space in terms of the modulation strength |η| and the comoving wavenumber ratio kl/ks, where PBH clusters can form and potentially explain the origin of LRDs (light-gray region) via run￾away mergers. The remaining regions represent param￾eter ranges where SMBHs at high redshift cannot form through mergers, as will be discussed in the following sections. FIG. 1: The |η|–(kl/ks) parameter plan… view at source ↗
Figure 2
Figure 2. FIG. 2: PBH mass population evolution in a cluster of [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3: Stochastic GW background from PBH cluster [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: FIG. 4: The PBH two-point correlation function for [PITH_FULL_IMAGE:figures/full_fig_p010_4.png]
Figure 5
Figure 5. Figure 5: FIG. 5: Redshift evolution of the most massive black hole in a PBH cluster of [PITH_FULL_IMAGE:figures/full_fig_p013_5.png]

Discussion (0). Sign in to comment.

Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Numerical simulations of primordial black hole formation via delayed first-order phase transitions

    gr-qc 2026-01 conditional novelty 6.0 of 10

    Spherically symmetric numerical relativity shows false-vacuum domains from delayed first-order phase transitions form type B (baby-universe) or type A (direct-collapse) primordial black holes, separated by a robust t_...

  2. Constraints on Primordial Black Hole Dressed by Dark Matter Halo from Microlensing Effect of Fast Radio Bursts

    astro-ph.CO 2026-07 conditional novelty 5.0 of 10

    A new conversion formula turns monochromatic bare-PBH microlensing bounds into extended-mass dressed-PBH bounds, and a 10^5-FRB forecast places f_PBH near 10^-4.

Reference graph

Works this paper leans on

111 extracted references · 5 canonical work pages · cited by 2 Pith papers

  1. [39]

    Heavy Primordial Black Holes from Strongly Clustered Light Black Holes,

    V. De Luca, G. Franciolini, and A. Riotto, “Heavy Primordial Black Holes from Strongly Clustered Light Black Holes,” Phys. Rev. Lett. 130 no. 17, (2023) 171401, arXiv:2210.14171 [astro-ph.CO]

    arXiv 2023

  2. [71]

    Zhang, W.-X

    B. Zhang, W.-X. Feng, and H. An. In preparation, 2025

    2025

  3. [1]

    Little Red Dots: An Abundant Population of Faint Active Galactic Nuclei at z∼ 5 Revealed by the EIGER and FRESCO JWST Surveys,

    J. Matthee et al., “Little Red Dots: An Abundant Population of Faint Active Galactic Nuclei at z∼ 5 Revealed by the EIGER and FRESCO JWST Surveys,” Astrophys. J. 963 no. 2, (2024) 129, arXiv:2306.05448 [astro-ph.GA]

    arXiv 2024

  4. [2]

    JWST CEERS and JADES Active Galaxies at z = 4–7 Violate the Local M•–M⋆ Relation at >3σ: Implications for Low-mass Black Holes and Seeding Models,

    F. Pacucci, B. Nguyen, S. Carniani, R. Maiolino, and X. Fan, “JWST CEERS and JADES Active Galaxies at z = 4–7 Violate the Local M•–M⋆ Relation at >3σ: Implications for Low-mass Black Holes and Seeding Models,” Astrophys. J. Lett. 957 no. 1, (2023) L3, arXiv:2308.12331 [astro-ph.GA]

    arXiv 2023

  5. [3]

    Not-so-little Red Dots: Two Massive and Dusty Starbursts at z∼ 5–7 Pushing the Limits of Star Formation Discovered by JWST in the COSMOS-Web Survey,

    F. Gentileet al., “Not-so-little Red Dots: Two Massive and Dusty Starbursts at z∼ 5–7 Pushing the Limits of Star Formation Discovered by JWST in the COSMOS-Web Survey,” Astrophys. J. Lett. 973 no. 1, (2024) L2, arXiv:2408.10305 [astro-ph.GA]

    arXiv 2024

  6. [4]

    Cosmos-web: The over-abundance and physical nature of

    H. B. Akins, C. M. Casey, E. Lambrides, N. Allen, I. T. Andika, M. Brinch, J. B. Champagne, O. Cooper, X. Ding, N. E. Drakos,et al., “Cosmos-web: The over-abundance and physical nature of" little red dots"–implications for early galaxy and smbh assembly,” arXiv:2406.10341 [astro-ph.GA]

    arXiv

  7. [5]

    The galaxies missed by hubble and alma: the contribution of extremely red galaxies to the cosmic census at 3< z< 8,

    C. C. Williams, S. Alberts, Z. Ji, K. N. Hainline, J. Lyu, G. Rieke, R. Endsley, K. A. Suess, F. Sun, B. D. Johnson,et al., “The galaxies missed by hubble and alma: the contribution of extremely red galaxies to the cosmic census at 3< z< 8,”Astrophys. J. 968 no. 1, (2024) 34,arXiv:2311.07483

    arXiv 2024

  8. [6]

    A JWST/NIRSpec First Census of Broad-Line AGNs at z = 4–7: Detection of 10 Faint AGNs with MBH ∼ 106–108Msun and Their Host Galaxy Properties,

    Y. Harikane, Y. Zhang, K. Nakajima, M. Ouchi, Y. Isobe, Y. Ono, S. Hatano, Y. Xu, and H. Umeda, “A JWST/NIRSpec First Census of Broad-Line AGNs at z = 4–7: Detection of 10 Faint AGNs with MBH ∼ 106–108Msun and Their Host Galaxy Properties,” Astrophys. J. 959 no. 1, (2023) 39, arXiv:2303.11946 [astro-ph.GA]

    arXiv 2023

Show all 111 references
  1. [7]

    JADES - The diverse population of infant black holes at 4< z < 11: Merging, tiny, poor, but mighty,

    R. Maiolinoet al., “JADES - The diverse population of infant black holes at 4< z < 11: Merging, tiny, poor, but mighty,” Astron. Astrophys. 691 (2024) A145, arXiv:2308.01230 [astro-ph.GA]

    2024 arXiv

  2. [8]

    Hidden little monsters: spectroscopic identification of low-mass, broad-line agns at z> 5 with ceers,

    D. D. Kocevski, M. Onoue, K. Inayoshi, J. R. Trump, 6 P. A. Haro, A. Grazian, M. Dickinson, S. L. Finkelstein, J. S. Kartaltepe, M. Hirschmann,et al., “Hidden little monsters: spectroscopic identification of low-mass, broad-line agns at z> 5 with ceers,” Astrophys.J.Lett.954 n...

    2023 arXiv

  3. [9]

    UNCOVER: A NIRSpec Identification of a Broad-line AGN at z = 8.50,

    V. Kokorev, S. Fujimoto, I. Labbe, J. E. Greene, R. Bezanson, P. Dayal, E. J. Nelson, H. Atek, G. Brammer, K. I. Caputi,et al., “UNCOVER: A NIRSpec Identification of a Broad-line AGN at z = 8.50,” Astrophys. J. Lett. 957 no. 1, (2023) L7, arXiv:2308.11610 [astro-ph.GA]

    2023 arXiv

  4. [10]

    Deciphering the jwst spectrum of a ‘little red dot’at z 4.53: An obscured agn and its star-forming host,

    M. Killi, D. Watson, G. Brammer, C. McPartland, J. Antwi-Danso, R. Newshore, D. Coe, N. Allen, J. P. Fynbo, K. Gould,et al., “Deciphering the jwst spectrum of a ‘little red dot’at z 4.53: An obscured agn and its star-forming host,”Astron. Astrophys. 691 (2024) A52, arXiv:2312....

    2024

  5. [11]

    A Census of Photometrically Selected Little Red Dots at 4 < z < 9 in JWST Blank Fields,

    V. Kokorev, K. I. Caputi, J. E. Greene, P. Dayal, M. Trebitsch, S. E. Cutler, S. Fujimoto, I. Labbé, T. B. Miller, E. Iani,et al., “A Census of Photometrically Selected Little Red Dots at 4 < z < 9 in JWST Blank Fields,”Astrophys. J. 968 no. 1, (2024) 38, arXiv:2401.09981 [ast...

    2024 arXiv

  6. [12]

    RUBIES: JWST/NIRSpec Confirmation of an Infrared-luminous, Broad-line Little Red Dot with an Ionized Outflow,

    B. Wang, A. de Graaff, R. L. Davies, J. E. Greene, J. Leja, G. B. Brammer, A. D. Goulding, T. B. Miller, K. A. Suess, A. Weibel,et al., “RUBIES: JWST/NIRSpec Confirmation of an Infrared-luminous, Broad-line Little Red Dot with an Ionized Outflow,” arXiv:2403.02304

    arXiv

  7. [13]

    Exploring the Active Galactic Nucleus Fraction of a Sample of JWST’s Little Red Dots at 4< z < 8: Overmassive Black Holes Are Strongly Favored,

    E. Durodola, F. Pacucci, and R. C. Hickox, “Exploring the Active Galactic Nucleus Fraction of a Sample of JWST’s Little Red Dots at 4< z < 8: Overmassive Black Holes Are Strongly Favored,”Astrophys. J. 985 no. 2, (2025) 169,arXiv:2406.10329 [astro-ph.GA]

    2025 arXiv

  8. [14]

    X-Ray View of Little Red Dots: Do They Host Supermassive Black Holes?,

    T. T. Ananna, A. Bogdán, O. E. Kovács, P. Natarajan, and R. C. Hickox, “X-Ray View of Little Red Dots: Do They Host Supermassive Black Holes?,”Astrophys. J. Lett.969 no. 1, (2024) L18,arXiv:2404.19010 [astro-ph.GA]

    2024 arXiv

  9. [15]

    The Rise of Faint, Red AGN at $z>4$: A Sample of Little Red Dots in the JWST Extragalactic Legacy Fields,

    D. D. Kocevski, S. L. Finkelstein, G. Barro, A. J. Taylor, A. Calabrò, B. Laloux, J. Buchner, J. R. Trump, G. C. Leung, G. Yang,et al., “The Rise of Faint, Red AGN at $z>4$: A Sample of Little Red Dots in the JWST Extragalactic Legacy Fields,” arXiv:2404.03576 [astro-ph.GA]

    arXiv

  10. [16]

    A high black-hole-to-host mass ratio in a lensed agn in the early universe,

    L. J. Furtak, I. Labbé, A. Zitrin, J. E. Greene, P. Dayal, I. Chemerynska, V. Kokorev, T. B. Miller, A. D. Goulding, A. de Graaff, R. Bezanson, G. B. Brammer, S. E. Cutler, J. Leja, R. Pan, S. H. Price, B. Wang, J. R. Weaver, K. E. Whitaker, H. Atek, Á. Bogdán, S. Charlot, E. ...

    2024 arXiv

  11. [17]

    A black hole in a near-pristine galaxy 700 million years after the Big Bang,

    R. Maiolino et al., “A black hole in a near-pristine galaxy 700 million years after the Big Bang,” arXiv:2505.22567 [astro-ph.GA]

    arXiv

  12. [18]

    Spin of Primordial Black Holes,

    M. Mirbabayi, A. Gruzinov, and J. Noreña, “Spin of Primordial Black Holes,”JCAP 03 (2020) 017, arXiv:1901.05963 [astro-ph.CO]

    2020 arXiv

  13. [19]

    The initial spin probability distribution of primordial black holes,

    V. De Luca, V. Desjacques, G. Franciolini, A. Malhotra, and A. Riotto, “The initial spin probability distribution of primordial black holes,” JCAP 05 (2019) 018, arXiv:1903.01179 [astro-ph.CO]

    2019 arXiv

  14. [20]

    Primordial black holes—perspectives in gravitational wave astronomy,

    M. Sasaki, T. Suyama, T. Tanaka, and S. Yokoyama, “Primordial black holes—perspectives in gravitational wave astronomy,” Class. Quant. Grav. 35 no. 6, (2018) 063001, arXiv:1801.05235 [astro-ph.CO]

    2018 arXiv

  15. [21]

    Constraints on primordial black holes,

    B. Carr, K. Kohri, Y. Sendouda, and J. Yokoyama, “Constraints on primordial black holes,”Rept. Prog. Phys. 84 no. 11, (2021) 116902,arXiv:2002.12778 [astro-ph.CO]

    2021 arXiv

  16. [22]

    Masses of quasars,

    A. Soltan, “Masses of quasars,”Mon. Not. Roy. Astron. Soc. 200 (1982) 115–122

    1982

  17. [23]

    Birth of Rapidly Spinning, Overmassive Black Holes in the Early Universe,

    K. Inayoshi and K. Ichikawa, “Birth of Rapidly Spinning, Overmassive Black Holes in the Early Universe,” Astrophys. J. Lett. 973 no. 2, (2024) L49, arXiv:2402.14706 [astro-ph.GA]

    2024 arXiv

  18. [24]

    LIGO/Virgo black holes and dark matter: The effect of spatial clustering,

    V. Atal, A. Sanglas, and N. Triantafyllou, “LIGO/Virgo black holes and dark matter: The effect of spatial clustering,”JCAP 11 (2020) 036, arXiv:2007.07212 [astro-ph.CO]

    2020 arXiv

  19. [25]

    Dynamical evolution of dense clusters of compact stars,

    G. D. Quinlan and S. L. Shapiro, “Dynamical evolution of dense clusters of compact stars,”Astrophys. J. 343 (1989) 725–749

    1989

  20. [26]

    Runaway merging of black holes: analytical constraint on the timescale,

    H. Mouri and Y. Taniguchi, “Runaway merging of black holes: analytical constraint on the timescale,” Astrophys. J. Lett. 566 (2002) L17–L20, arXiv:astro-ph/0201102

    2002 arXiv

  21. [27]

    Gravitational Waves from Primordial Black Hole Dark Matter Spikes,

    W.-X. Feng, S. Bird, and H.-B. Yu, “Gravitational Waves from Primordial Black Hole Dark Matter Spikes,” Astrophys. J. 986 no. 2, (2025) 151, arXiv:2411.05065 [astro-ph.CO]

    2025 arXiv

  22. [28]

    Inhomogeneous non-Gaussianity,

    C. T. Byrnes, S. Nurmi, G. Tasinato, and D. Wands, “Inhomogeneous non-Gaussianity,” JCAP 03 (2012) 012, arXiv:1111.2721 [astro-ph.CO]

    2012 arXiv

  23. [29]

    Primordial black holes as a tool for constraining non-Gaussianity,

    C. T. Byrnes, E. J. Copeland, and A. M. Green, “Primordial black holes as a tool for constraining non-Gaussianity,” Phys. Rev. D 86 (2012) 043512, arXiv:1206.4188 [astro-ph.CO]

    2012 arXiv

  24. [30]

    Primordial black holes in non-Gaussian regimes,

    S. Young and C. T. Byrnes, “Primordial black holes in non-Gaussian regimes,” JCAP 08 (2013) 052, arXiv:1307.4995 [astro-ph.CO]

    2013 arXiv

  25. [31]

    Long-short wavelength mode coupling tightens primordial black hole constraints,

    S. Young and C. T. Byrnes, “Long-short wavelength mode coupling tightens primordial black hole constraints,” Phys. Rev. D 91 no. 8, (2015) 083521, arXiv:1411.4620 [astro-ph.CO]

    2015 arXiv

  26. [32]

    Signatures of non-gaussianity in the isocurvature modes of primordial black hole dark matter,

    S. Young and C. T. Byrnes, “Signatures of non-gaussianity in the isocurvature modes of primordial black hole dark matter,”JCAP 04 (2015) 034, arXiv:1503.01505 [astro-ph.CO]

    2015 arXiv

  27. [33]

    Primordial black holes as biased tracers,

    Y. Tada and S. Yokoyama, “Primordial black holes as biased tracers,” Phys. Rev. D 91 no. 12, (2015) 123534, arXiv:1502.01124 [astro-ph.CO]

    2015 arXiv

  28. [34]

    Primordial Black Holes from Inflation and non-Gaussianity,

    G. Franciolini, A. Kehagias, S. Matarrese, and A. Riotto, “Primordial Black Holes from Inflation and non-Gaussianity,” JCAP 03 (2018) 016, arXiv:1801.09415 [astro-ph.CO]

    2018 arXiv

  29. [35]

    Spatial clustering of primordial black holes,

    V. Desjacques and A. Riotto, “Spatial clustering of primordial black holes,”Phys. Rev. D 98 no. 12, (2018) 123533, arXiv:1806.10414 [astro-ph.CO]

    2018 arXiv

  30. [36]

    Correlation Function of 7 High-Threshold Regions and Application to the Initial Small-Scale Clustering of Primordial Black Holes,

    Y. Ali-Haïmoud, “Correlation Function of 7 High-Threshold Regions and Application to the Initial Small-Scale Clustering of Primordial Black Holes,” Phys. Rev. Lett. 121 no. 8, (2018) 081304, arXiv:1805.05912 [astro-ph.CO]

    2018 arXiv

  31. [37]

    Initial clustering and the primordial black hole merger rate,

    S. Young and C. T. Byrnes, “Initial clustering and the primordial black hole merger rate,”JCAP 03 (2020) 004, arXiv:1910.06077 [astro-ph.CO]

    2020 arXiv

  32. [38]

    Clustering of primordial black holes with non-Gaussian initial fluctuations,

    T. Suyama and S. Yokoyama, “Clustering of primordial black holes with non-Gaussian initial fluctuations,” PTEP 2019 no. 10, (2019) 103E02, arXiv:1906.04958 [astro-ph.CO]

    2019 arXiv

  33. [40]

    Ruling Out Initially Clustered Primordial Black Holes as Dark Matter,

    V. De Luca, G. Franciolini, A. Riotto, and H. Veermäe, “Ruling Out Initially Clustered Primordial Black Holes as Dark Matter,”Phys. Rev. Lett. 129 no. 19, (2022) 191302, arXiv:2208.01683 [astro-ph.CO]

    2022 arXiv

  34. [41]

    Primordial structure of massive black hole clusters,

    M. Y. Khlopov, S. G. Rubin, and A. S. Sakharov, “Primordial structure of massive black hole clusters,” Astropart. Phys. 23 (2005) 265, arXiv:astro-ph/0401532

    2005 arXiv

  35. [42]

    Quasars formation around clusters of primordial black holes,

    V. Dokuchaev, Y. Eroshenko, and S. Rubin, “Quasars formation around clusters of primordial black holes,” Grav. Cosmol. 11 (2005) 99–104, arXiv:astro-ph/0412418

    2005 arXiv

  36. [43]

    Clusters of primordial black holes,

    K. M. Belotsky, V. I. Dokuchaev, Y. N. Eroshenko, E. A. Esipova, M. Y. Khlopov, L. A. Khromykh, A. A. Kirillov, V. V. Nikulin, S. G. Rubin, and I. V. Svadkovsky, “Clusters of primordial black holes,”Eur. Phys. J. C 79 no. 3, (2019) 246,arXiv:1807.06590 [astro-ph.CO]

    2019 arXiv

  37. [44]

    Detectability of Gravitational Waves from the Coalescence of Massive Primordial Black Holes with Initial Clustering,

    Q. Ding, T. Nakama, J. Silk, and Y. Wang, “Detectability of Gravitational Waves from the Coalescence of Massive Primordial Black Holes with Initial Clustering,” Phys. Rev. D 100 no. 10, (2019) 103003, arXiv:1903.07337 [astro-ph.CO]

    2019 arXiv

  38. [45]

    Toward supermassive primordial black holes from inflationary bubbles,

    H.-L. Huang and Y.-S. Piao, “Toward supermassive primordial black holes from inflationary bubbles,” Phys. Rev. D 110 no. 2, (2024) 023501, arXiv:2312.11982 [astro-ph.CO]

    2024 arXiv

  39. [46]

    Primordial black holes from fifth forces,

    L. Amendola, J. Rubio, and C. Wetterich, “Primordial black holes from fifth forces,”Phys. Rev. D 97 no. 8, (2018) 081302, arXiv:1711.09915 [astro-ph.CO]

    2018 arXiv

  40. [47]

    Primordial dark matter halos from fifth forces,

    S. Savastano, L. Amendola, J. Rubio, and C. Wetterich, “Primordial dark matter halos from fifth forces,” Phys. Rev. D 100 no. 8, (2019) 083518, arXiv:1906.05300 [astro-ph.CO]

    2019 arXiv

  41. [48]

    Primordial Black Holes from Long-Range Scalar Forces and Scalar Radiative Cooling,

    M. M. Flores and A. Kusenko, “Primordial Black Holes from Long-Range Scalar Forces and Scalar Radiative Cooling,” Phys. Rev. Lett. 126 no. 4, (2021) 041101, arXiv:2008.12456 [astro-ph.CO]

    2021 arXiv

  42. [49]

    The exponential tail of inflationary fluctuations: consequences for primordial black holes,

    J. M. Ezquiaga, J. García-Bellido, and V. Vennin, “The exponential tail of inflationary fluctuations: consequences for primordial black holes,”JCAP 03 (2020) 029, arXiv:1912.05399 [astro-ph.CO]

    2020 arXiv

  43. [50]

    Massive Galaxy Clusters Like El Gordo Hint at Primordial Quantum Diffusion,

    J. M. Ezquiaga, J. García-Bellido, and V. Vennin, “Massive Galaxy Clusters Like El Gordo Hint at Primordial Quantum Diffusion,”Phys. Rev. Lett. 130 no. 12, (2023) 121003,arXiv:2207.06317 [astro-ph.CO]

    2023 arXiv

  44. [51]

    Clustering of primordial black holes from quantum diffusion during inflation,

    C. Animali and V. Vennin, “Clustering of primordial black holes from quantum diffusion during inflation,” JCAP 08 (2024) 026, arXiv:2402.08642 [astro-ph.CO]

    2024 arXiv

  45. [52]

    Bubble correlation in first-order phase transitions,

    V. De Luca, G. Franciolini, and A. Riotto, “Bubble correlation in first-order phase transitions,”Phys. Rev. D 104 no. 12, (2021) 123539,arXiv:2110.04229 [hep-ph]

    2021 arXiv

  46. [53]

    Threshold of primordial black hole formation,

    T. Harada, C.-M. Yoo, and K. Kohri, “Threshold of primordial black hole formation,”Phys. Rev. D 88 no. 8, (2013) 084051,arXiv:1309.4201 [astro-ph.CO]. [Erratum: Phys.Rev.D 89, 029903 (2014)]

    2013 arXiv

  47. [54]

    Drei Vortrage uber Diffusion, Brownsche Bewegung und Koagulation von Kolloidteilchen,

    M. V. Smoluchowski, “Drei Vortrage uber Diffusion, Brownsche Bewegung und Koagulation von Kolloidteilchen,” Zeitschrift für Physik 17 (1916) 557–585

    1916

  48. [55]

    Versuch einer mathematischen theorie der koagulationskinetik kolloider lösungen,

    M. V. Smoluchowski, “Versuch einer mathematischen theorie der koagulationskinetik kolloider lösungen,” Zeitschrift für Physikalische Chemie 92 no. 1, (1917) 129–168. http://dx.doi.org/10.1515/zpch-1918-9209

    1917 doi

  49. [56]

    Stochastic problems in physics and astronomy,

    S. Chandrasekhar, “Stochastic problems in physics and astronomy,” Rev. Mod. Phys. 15 (1943) 1–89

    1943

  50. [57]

    Large amplitude isothermal fluctuations and high density dark matter clumps,

    E. W. Kolb and I. I. Tkachev, “Large amplitude isothermal fluctuations and high density dark matter clumps,” Phys. Rev. D 50 (1994) 769–773, arXiv:astro-ph/9403011

    1994 arXiv

  51. [58]

    Hoop conjecture for black-hole horizon formation,

    E. Flanagan, “Hoop conjecture for black-hole horizon formation,” Phys. Rev. D 44 no. 8, (1991) 2409–2420

    1991

  52. [59]

    The Most Probable Phase Distribution in Spherical Stellar Systems and the Conditions Governing Its Existence,

    V. A. Antonov, “The Most Probable Phase Distribution in Spherical Stellar Systems and the Conditions Governing Its Existence,”

  53. [60]

    The Gravo-Thermal Catastrophe in Isothermal Spheres and the Onset of Red-Giant Structure for Stellar Systems,

    D. Lynden-Bell, R. Wood, and A. Royal, “The Gravo-Thermal Catastrophe in Isothermal Spheres and the Onset of Red-Giant Structure for Stellar Systems,” Mon. Not. Roy. Astron. Soc. 138 no. 4, (1968) 495–525

    1968

  54. [61]

    Antonov instability and gravothermal catastrophe-revisited,

    T. Padmanabhan, “Antonov instability and gravothermal catastrophe-revisited,” Astrophys. J. Suppl. 71 (1989) 651–664

    1989

  55. [62]

    Gravitational instability of finite isothermal spheres,

    P.-H. Chavanis, “Gravitational instability of finite isothermal spheres,” Astron. Astrophys. 381 (2002) 340, arXiv:astro-ph/0103159

    2002 arXiv

  56. [63]

    The stochastic coalescence model for cloud droplet growth,

    D. T. Gillespie, “The stochastic coalescence model for cloud droplet growth,”J. Atmos. Sci. 29 no. 8, (1972) 1496–1510

    1972

  57. [64]

    An exact method for numerically simulating the stochastic coalescence process in a cloud,

    D. T. Gillespie, “An exact method for numerically simulating the stochastic coalescence process in a cloud,” J. Atmos. Sci. 32 no. 10, (1975) 1977–1989

    1975

  58. [65]

    A Monte Carlo simulation of coagulation,

    A. L. Garcia, C. Van Den Broeck, M. Aertsens, and R. Serneels, “A Monte Carlo simulation of coagulation,” Phys. A: Stat. Mech. Appl. 143 no. 3, (1987) 535–546

    1987

  59. [66]

    A direct simulation Monte-Carlo method for cluster coagulation,

    K. Liffman, “A direct simulation Monte-Carlo method for cluster coagulation,” J. Comput. Phys. 100 no. 1, (1992) 116–127

    1992

  60. [67]

    On a Monte Carlo scheme for Smoluchowski’s coagulation equation,

    H. Babovsky, “On a Monte Carlo scheme for Smoluchowski’s coagulation equation,”Monte Carlo Methods Appl. 5 no. 1, (1999) 1–18

    1999

  61. [68]

    Stochastic weighted particle methods for population balance equations,

    R. I. Patterson, W. Wagner, and M. Kraft, “Stochastic weighted particle methods for population balance equations,” J. Comput. Phys. 230 no. 19, (2011) 7456–7472

    2011

  62. [69]

    A Monte Carlo method for the simulation of coagulation and nucleation based 8 on weighted particles and the concepts of stochastic resolution and merging,

    G. Kotalczyk and F. Kruis, “A Monte Carlo method for the simulation of coagulation and nucleation based 8 on weighted particles and the concepts of stochastic resolution and merging,” J. Comput. Phys. 340 (2017) 276–296

    2017

  63. [70]

    Fragmentation and entanglement limit vimentin intermediate filament assembly,

    Q. D. Tran, V. Sorichetti, G. Pehau-Arnaudet, M. Lenz, and C. Leduc, “Fragmentation and entanglement limit vimentin intermediate filament assembly,” Phys. Rev. X 13 no. 1, (2023) 011014

    2023

  64. [72]

    LISA Definition Study Report,

    M. Colpi et al., “LISA Definition Study Report,” arXiv:2402.07571 [astro-ph.CO]

    arXiv

  65. [73]

    Taiji program: Gravitational-wave sources,

    W.-H. Ruan, Z.-K. Guo, R.-G. Cai, and Y.-Z. Zhang, “Taiji program: Gravitational-wave sources,”Int. J. Mod. Phys. A 35 no. 17, (2020) 2050075, arXiv:1807.09495 [gr-qc]

    2020 arXiv

  66. [74]

    The TianQin project: current progress on science and technology,

    TianQin Collaboration, J. Meiet al., “The TianQin project: current progress on science and technology,” PTEP 2021 no. 5, (2021) 05A107,arXiv:2008.10332 [gr-qc]

    2021

  67. [75]

    Detecting a gravitational-wave background with next-generation space interferometers,

    H. Kudoh, A. Taruya, T. Hiramatsu, and Y. Himemoto, “Detecting a gravitational-wave background with next-generation space interferometers,” Phys. Rev. D 73 (2006) 064006, arXiv:gr-qc/0511145

    2006 arXiv

  68. [76]

    Current status of space gravitational wave antenna DECIGO and B-DECIGO,

    S. Kawamuraet al., “Current status of space gravitational wave antenna DECIGO and B-DECIGO,” PTEP 2021 no. 5, (2021) 05A105, arXiv:2006.13545 [gr-qc]

    2021 arXiv

  69. [77]

    The Science of the Einstein Telescope,

    A. Abac et al., “The Science of the Einstein Telescope,” arXiv:2503.12263 [gr-qc]

    arXiv

  70. [78]

    Upper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo’s third observing run,

    KAGRA, Virgo, LIGO ScientificCollaboration, R. Abbott et al., “Upper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo’s third observing run,”Phys. Rev. D 104 no. 2, (2021) 022004,arXiv:2101.12130 [gr-qc]

    2021

  71. [79]

    Rotating black holes: Locally nonrotating frames, energy extraction, and scalar synchrotron radiation,

    J. M. Bardeen, W. H. Press, and S. A. Teukolsky, “Rotating black holes: Locally nonrotating frames, energy extraction, and scalar synchrotron radiation,” Astrophys. J. 178 (1972) 347

    1972

  72. [80]

    Spin, accretion and the cosmological growth of supermassive black holes,

    S. L. Shapiro, “Spin, accretion and the cosmological growth of supermassive black holes,”Astrophys. J. 620 (2005) 59–68, arXiv:astro-ph/0411156

    2005 arXiv

  73. [81]

    The Evolution of Black Hole Mass and Spin in Active Galactic Nuclei,

    A. R. King, J. E. Pringle, and J. A. Hofmann, “The Evolution of Black Hole Mass and Spin in Active Galactic Nuclei,” Mon. Not. Roy. Astron. Soc. 385 (2008) 1621, arXiv:0801.1564 [astro-ph]

    2008 arXiv

  74. [82]

    Supermassive black hole spin evolution in cosmological simulations with OPENGADGET3,

    L. Sala, M. Valentini, V. Biffi, and K. Dolag, “Supermassive black hole spin evolution in cosmological simulations with OPENGADGET3,” Astron. Astrophys. 685 (2024) A92, arXiv:2312.07657 [astro-ph.GA]

    2024 arXiv

  75. [83]

    Primordial black hole formation from a nonspherical density profile with a misaligned deformation tensor,

    C.-M. Yoo, “Primordial black hole formation from a nonspherical density profile with a misaligned deformation tensor,” Phys. Rev. D 110 no. 4, (2024) 043526, arXiv:2403.11147 [gr-qc]

    2024 arXiv

  76. [84]

    Origin of the Angular Momentum of Galaxies,

    P. J. E. Peebles, “Origin of the Angular Momentum of Galaxies,” Astrophys. J. 155 (1969) 393

    1969

  77. [85]

    The Statistics of Peaks of Gaussian Random Fields,

    J. M. Bardeen, J. R. Bond, N. Kaiser, and A. S. Szalay, “The Statistics of Peaks of Gaussian Random Fields,” Astrophys. J. 304 (1986) 15–61

    1986

  78. [86]

    Ellipsoidal collapse and an improved model for the number and spatial distribution of dark matter haloes,

    R. K. Sheth, H. J. Mo, and G. Tormen, “Ellipsoidal collapse and an improved model for the number and spatial distribution of dark matter haloes,”Mon. Not. Roy. Astron. Soc. 323 (2001) 1, arXiv:astro-ph/9907024

    2001 arXiv

  79. [87]

    Simulations of Ellipsoidal Primordial Black Hole Formation,

    A. Escrivà and C.-M. Yoo, “Simulations of Ellipsoidal Primordial Black Hole Formation,”arXiv:2410.03452 [gr-qc]

  80. [88]

    Primordial Black Holes as Dark Matter,

    B. Carr, F. Kuhnel, and M. Sandstad, “Primordial Black Holes as Dark Matter,”Phys. Rev. D 94 no. 8, (2016) 083504, arXiv:1607.06077 [astro-ph.CO]

    2016 arXiv

  81. [89]

    New X-ray bound on density of primordial black holes,

    Y. Inoue and A. Kusenko, “New X-ray bound on density of primordial black holes,”JCAP 10 (2017) 034, arXiv:1705.00791 [astro-ph.CO]

    2017 arXiv

  82. [90]

    Dynamical constraints on dark compact objects,

    B. J. Carr and M. Sakellariadou, “Dynamical constraints on dark compact objects,”Astrophys. J. 516 (1999) 195–220

    1999

  83. [91]

    Probing the inflaton: Small-scale power spectrum constraints from measurements of the CMB energy spectrum,

    J. Chluba, A. L. Erickcek, and I. Ben-Dayan, “Probing the inflaton: Small-scale power spectrum constraints from measurements of the CMB energy spectrum,” Astrophys. J. 758 (2012) 76, arXiv:1203.2681 [astro-ph.CO]

    2012 arXiv

  84. [92]

    CMB at 2x2 order: The dissipation of primordial acoustic waves and the observable part of the associated energy release,

    J. Chluba, R. Khatri, and R. A. Sunyaev, “CMB at 2x2 order: The dissipation of primordial acoustic waves and the observable part of the associated energy release,” Mon. Not. Roy. Astron. Soc. 425 (2012) 1129–1169, arXiv:1202.0057 [astro-ph.CO]

    2012 arXiv

  85. [93]

    Primordial seeds of supermassive black holes,

    M. Kawasaki, A. Kusenko, and T. T. Yanagida, “Primordial seeds of supermassive black holes,”Phys. Lett. B 711 (2012) 1–5, arXiv:1202.3848 [astro-ph.CO]

    2012 arXiv

  86. [94]

    Testing scenarios of primordial black holes being the seeds of supermassive black holes by ultracompact minihalos and CMB µ-distortions,

    K. Kohri, T. Nakama, and T. Suyama, “Testing scenarios of primordial black holes being the seeds of supermassive black holes by ultracompact minihalos and CMB µ-distortions,” Phys. Rev. D 90 no. 8, (2014) 083514, arXiv:1405.5999 [astro-ph.CO]

    2014 arXiv

  87. [95]

    Limits on primordial black holes fromµ distortions in cosmic microwave background,

    T. Nakama, B. Carr, and J. Silk, “Limits on primordial black holes fromµ distortions in cosmic microwave background,” Phys. Rev. D 97 no. 4, (2018) 043525, arXiv:1710.06945 [astro-ph.CO]

    2018 arXiv

  88. [96]

    The Cosmic Microwave Background spectrum from the full COBE FIRAS data set,

    D. J. Fixsen, E. S. Cheng, J. M. Gales, J. C. Mather, R. A. Shafer, and E. L. Wright, “The Cosmic Microwave Background spectrum from the full COBE FIRAS data set,”Astrophys. J. 473 (1996) 576, arXiv:astro-ph/9605054

    1996 arXiv

  89. [97]

    Dynamical instability of collapsed dark matter halos,

    W.-X. Feng, H.-B. Yu, and Y.-M. Zhong, “Dynamical instability of collapsed dark matter halos,”JCAP 05 no. 05, (2022) 036,arXiv:2108.11967 [astro-ph.CO]

    2022 arXiv

  90. [98]

    Pushing towards the ET sensitivity using ’conventional’ technology,

    S. Hild, S. Chelkowski, and A. Freise, “Pushing towards the ET sensitivity using ’conventional’ technology,” arXiv:0810.0604 [gr-qc]

    arXiv

  91. [99]

    Beyond the Second Generation of Laser-Interferometric Gravitational Wave Observatories,

    S. Hild, “Beyond the Second Generation of Laser-Interferometric Gravitational Wave Observatories,” Class. Quant. Grav. 29 (2012) 124006, arXiv:1111.6277 [gr-qc]

    2012 arXiv

  92. [100]

    Exploring compact binary populations with the Einstein Telescope,

    N. Singh, T. Bulik, K. Belczynski, and A. Askar, “Exploring compact binary populations with the Einstein Telescope,” Astron. Astrophys. 667 (2022) A2, arXiv:2112.04058 [astro-ph.HE]

    2022 arXiv

  93. [101]

    Supermassive primordial black holes from inflation,

    D. Hooper, A. Ireland, G. Krnjaic, and A. Stebbins, “Supermassive primordial black holes from inflation,” JCAP 04 (2024) 021, arXiv:2308.00756 [astro-ph.CO]

    2024 arXiv

  94. [102]

    Not-quite-primordial black holes,

    W. Qin, S. Kumar, P. Natarajan, and N. Weiner, “Not-quite-primordial black holes,” arXiv:2506.13858 [astro-ph.CO]

    arXiv

  95. [103]

    Seeding 9 Supermassive Black Holes with Self-interacting Dark Matter: A Unified Scenario with Baryons,

    W.-X. Feng, H.-B. Yu, and Y.-M. Zhong, “Seeding 9 Supermassive Black Holes with Self-interacting Dark Matter: A Unified Scenario with Baryons,”Astrophys. J. Lett. 914 no. 2, (2021) L26,arXiv:2010.15132 [astro-ph.CO]

    2021 arXiv

  96. [104]

    Early formation of supermassive black holes from the collapse of strongly self-interacting dark matter,

    M. G. Roberts, L. Braff, A. Garg, S. Profumo, T. Jeltema, and J. O’Donnell, “Early formation of supermassive black holes from the collapse of strongly self-interacting dark matter,”JCAP 01 (2025) 060, arXiv:2410.17480 [astro-ph.GA]

    2025 arXiv

  97. [105]

    Formation of the Little Red Dots from the Core-collapse of Self-interacting Dark Matter Halos,

    F. Jiang, Z. Jia, H. Zheng, L. C. Ho, K. Inayoshi, X. Shen, M. Vogelsberger, and W.-X. Feng, “Formation of the Little Red Dots from the Core-collapse of Self-interacting Dark Matter Halos,” arXiv:2503.23710 [astro-ph.GA]

  98. [106]

    Massive Black Holes Seeded by Dark Matter – Implications for Little Red Dots and Gravitational Wave Signatures,

    T. Shen, X. Shen, H. Xiao, M. Vogelsberger, and F. Jiang, “Massive Black Holes Seeded by Dark Matter – Implications for Little Red Dots and Gravitational Wave Signatures,” arXiv:2504.00075 [astro-ph.GA]

    arXiv

  99. [107]

    Dark Bondi Accretion Aided by Baryons and the Origin of JWST Little Red Dots,

    W.-X. Feng, H.-B. Yu, and Y.-M. Zhong, “Dark Bondi Accretion Aided by Baryons and the Origin of JWST Little Red Dots,”arXiv:2506.17641 [astro-ph.GA]

    arXiv

  100. [108]

    Little Red Dots from Ultra-Strongly Self-Interacting Dark Matter,

    M. G. Roberts, L. Braff, A. Garg, S. Profumo, and T. Jeltema, “Little Red Dots from Ultra-Strongly Self-Interacting Dark Matter,”arXiv:2507.03230 [astro-ph.GA]

  101. [109]

    Primordial Black Holes as Generators of Cosmic Structures,

    B. Carr and J. Silk, “Primordial Black Holes as Generators of Cosmic Structures,”Mon. Not. Roy. Astron. Soc. 478 no. 3, (2018) 3756–3775, arXiv:1801.00672 [astro-ph.CO]

    2018 arXiv

  102. [110]

    An inflation model for massive primordial black holes to interpret the JWST observations,

    B.-Y. Su, N. Li, and L. Feng, “An inflation model for massive primordial black holes to interpret the JWST observations,” arXiv:2306.05364 [astro-ph.CO]

    arXiv

  103. [111]

    The properties of primordially-seeded black holes and their hosts in the first billion years: implications for JWST,

    P. Dayal and R. maiolino, “The properties of primordially-seeded black holes and their hosts in the first billion years: implications for JWST,” arXiv:2506.08116 [astro-ph.GA] . 1 — Supplemental Material — Little Red Dots from Small-Scale Primordial Black Hole Clustering Borui...

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.